Ever since the first star in the Universe ignited some 13.7 billion years ago, the Universe has been flooded with light. When enough matter — mostly hydrogen and helium gas — gravitates together into a single, compact object, nuclear fusion will take place inside the core, giving rise to a true star. But as time goes on and fusion continues, eventually that star will run out of fuel. Sometimes, the star is massive enough that additional fusion reactions will take place, but at some point, it all must stop. When those stars finally die, however, their remnants shine on. In fact, the Universe hasn't been around long enough for even a single remnant to stop shining. Here's the story of how long we'll need to wait for the first star to go dark.

It all begins from a cloud of gas. When a cloud of molecular gas collapses under its own gravity, there are always a few regions that start off just a little bit denser than others. Every location with matter in it does its best to attract more and more matter towards it, but these overdense regions attract matter more efficiently than all the others. Because gravitational collapse is a runaway process, the more matter you attract to your vicinity, the faster additional matter accelerates to join you.

Dark, dusty molecular clouds, like this one within our Milky Way, will collapse over time and give rise to new stars, with the densest regions within forming the most massive stars.

(ESO)

While it can take millions to tens of millions of years for a molecular cloud to go from a large, diffuse state to a relatively collapsed one, the process of going from a collapsed state of dense gas to a new cluster of stars — where the densest regions ignite fusion in their cores — takes only a few hundred thousand years.

Stars come in a huge variety of colors, brightnesses and masses, all of which are predestined from the moment of the star's birth. When you create a new cluster of stars, the easiest ones to notice are the brightest ones, which also happen to be the most massive. These are the brightest, bluest, hottest stars in existence, with up to hundreds of times the mass of our Sun and with millions of times the luminosity. But despite the fact that these are the stars that appear the most spectacular, these are also the rarest stars, making up far less than 1% of all the known, total stars, and also the shortest-lived stars, as they burn through all the nuclear fuel (in all the various stages) in their cores in as little as 1–2 million years.

Hubble space telescope of the merging star clusters at the heart of the Tarantula Nebula, the largest star-forming region known in the local group. The hottest, bluest stars are over 200 times the mass of our Sun. [NASA, ESA, and E. Sabbi (ESA/STScI); Acknowledgment: R. O'Connell (University of Virginia) and the Wide Field Camera 3 Science Oversight Committee]

When these brightest stars run out of fuel, they die in a spectacular type II supernova explosion. As this occurs, the inner core implodes, collapsing all the way down to a neutron star (for the low-mass cores) or even to a black hole (for the high-mass cores), while expelling the outer layers back into the interstellar medium. There, these enriched gases will contribute to future generations of stars, providing them with the heavy elements necessary to create rocky planets, organic molecules, and in rare, wonderful cases, life.

When the most massive stars die, their outer layers, enriched with heavy elements from the result of nuclear fusion and neutron capture, are blown off into the interstellar medium, where they can help future generations of starsby providing them with the raw ingredients for rocky planets and, potentially, life. [NASA, ESA, J. Hester, A. Loll (ASU)]

You don't have to wait long for a black hole to go dark. In fact, by definition, black holes go "black" immediately. Once the core collapses sufficiently to form an event horizon, everything inside collapses down to a singularity in a fraction of a second. Any remnant heat, light, temperature, or energy in any form in the core simply gets converted into the mass of the singularity. No light will ever emanate from it again, except in the form of Hawking radiation, when the black hole decays, and in the accretion disk surrounding the black hole, which is constantly fed and refueled from the surrounding matter.

But neutron stars are a different story.

Forming from the remnant of a massive star that's gone supernova, a neutron star is the collapsed core that remains behind.

(NASA)

You see, a neutron star takes all the energy in a star’s core and collapses incredibly rapidly. When you take anything and compress it quickly, you cause the temperature within it to rise: this is how a piston works in a diesel engine. Well, collapsing from a stellar core all the way down to a neutron star is maybe the ultimate example of rapid compression. In the span of seconds-to-minutes, a core of iron, nickel, cobalt, silicon and sulfur many hundreds-of-thousands of miles (kilometers) in diameter has collapsed down to a ball just around 10 miles (16 km) in size or smaller. Its density has increased by around a factor of a quadrillion (10^15), and its temperature has grown tremendously: to some 10^12 K in the core and all the way up to around 10^6 K at the surface. And herein lies the problem.

A neutron star is very small and low in overall luminosity, but it's very hot, and takes a long time to cool down. If your eyes were good enough, you'd see it shine for millions of times the present age of the Universe.(ESO/L. Calçada)

You have all this energy stored within a collapsed star like this, and its surface is so tremendously hot that it not only glows bluish-white in the visible portion of the spectrum, but most of the energy isn’t visible or even ultraviolet: it’s X-ray energy! There is an insanely large amount of energy stored within this object, but the only way it can release it out into the Universe is through its surface, and its surface area is very small. The big question, of course, is how long will it take a neutron star to cool?

The answer depends on a piece of physics that practically isn’t well-understood for neutron stars: neutrino cooling! You see, while photons (radiation) are soundly trapped by the normal, baryonic matter, neutrinos, when generated, can pass right through the entire neutron star unimpeded. On the fast end, neutron stars might cool down, out of the visible portion of the spectrum, after as little as 10^16 years, or “only” a million times the age of the Universe. But if things are slower, it might take 10^20-to-10^22 years, which means you’ll be waiting for some time.

When lower-mass, Sun-like stars run out of fuel, they blow off their outer layers in a planetary nebula, but the center contracts down to form a white dwarf, which takes a very long time to fade to darkness. [NASA/ESA and The Hubble Heritage Team (AURA/STScI)]

But other stars will go dark much more quickly. You see, the vast majority of stars — the other 99+% — don’t go supernova, but rather, at the end of their lives, contract (slowly) down into a white dwarf star. The “slow” timescale is only slow compared to a supernova: it takes tens-to-hundreds of thousands of years rather than mere seconds-to-minutes, but that’s still fast enough to trap almost all the heat from the star’s core inside. The big difference is that instead of trapping it inside of a sphere with a diameter of only 10 miles or so, the heat is trapped in an object “only” about the size of Earth, or around a thousand times larger than a neutron star. This means that while the temperatures of these white dwarfs can be very high — over 20,000 K, or more than three times hotter than our Sun — they cool down much faster than neutron stars.

Neutrino escape is negligible in white dwarfs, meaning that radiation through the surface is the only effect that matters. When we calculate how quickly heat can escape by radiating away, it leads to a cooling timescale for a white dwarf (like the kind the Sun will produce) of around 10^14-to-10^15 years. And that’s to get all the way down to just a few degrees above absolute zero! This means that after around 10 trillion years, or “only” around 1,000 times the present age of the Universe, the surface of a white dwarf will have dropped in temperature so that it’s out of the visible light regime. When this much time has passed, the Universe will possess a brand new type of object: a black dwarf star.

The Universe is not yet old enough for a stellar remnant to have cooled enough to become invisible to human eyes, much less to cool all the way to just a few degrees above absolute zero.

(NASA / JPL-Caltech)

I’m sorry to disappoint you, but there aren’t any black dwarfs around today. The Universe is simply far too young for it. In fact, the coolest white dwarfs have, to the best of our estimates, lost less than 0.2% of their total heat since the very first ones were created in this Universe. For a white dwarf created at 20,000 K, that means its temperature is still at least 19,960 K, telling us we’ve got a terribly long way to go, if we’re waiting for a true dark star.

We currently conceive of our Universe as littered with stars, which cluster together into galaxies, which are separated by vast distances. But by time the first black dwarf comes to be, our local group will have merged into a single galaxy (Milkdromeda), most of the stars that will ever live will have long since burned out, with the surviving ones being exclusively the lowest-mass, reddest and dimmest stars of all. And beyond that? Only darkness, as dark energy will have long since pushed away all the other galaxies, making them unreachable and practically unmeasureable by any physical means.

It will take hundreds of trillions of years for the first stellar remnant to cool completely, fading from a white dwarf through red, infrared and all the way down to a true black dwarf. By that point, the Universe will hardly be forming any new stars at all, and space will be mostly black. (user Toma/Space Engine; E. Siegel)

And yet, amidst it all, a new type of object will come to be for the very first time. Even though we’ll never see or experience one, we know enough of nature to know not only that they’ll exist, but how and when they’ll come to be. And that, in itself, is one of the most amazing parts of science of all!